11,180 research outputs found
Entanglement Detection by Local Orthogonal Observables
We propose a family of entanglement witnesses and corresponding positive maps
that are not completely positive based on local orthogonal observables. As
applications the entanglement witness of the bound entangled state
[P. Horodecki, Phys. Lett. A {\bf 232}, 333 (1997)] is explicitly constructed
and a family of -dimensional bound entangled states is designed so that the
entanglement can be detected by permuting local orthogonal observables. Further
the proposed physically not implementable positive maps can be physically
realized by measuring a Hermitian correlation matrix of local orthogonal
observables.Comment: 4 pages, 1 figur
Flexural properties of fiber reinforced root canal posts.
AbstractOBJECTIVES: Fiber-reinforced
composite (FRC) root canal posts have been introduced to be used
instead of metal alloys and ceramics. The aim of this study was to
investigate the flexural properties of different types of FRC posts and
compare those values with a novel FRC material for dental applications.METHODS: Seventeen
different FRC posts of various brands (Snowpost, Carbopost, Parapost,
C-post, Glassix, Carbonite) and diameters, (1.0-2.1 mm) and a continuous
unidirectional E-glass FRC polymerized by light activation to a
cylindrical form (everStick, diameter 1.5 mm) as a control material were
tested. The posts (n=5) were stored at room's humidity or thermocycled
(12.000 x, 5 degrees C/55 degrees C) and stored in water for 2 weeks
before testing. A three-point bending test (span=10 mm) was used to
measure the flexural strength and modulus of FRC post specimens.RESULTS: Analysis
of ANOVA revealed that thermocycling, brand of material and diameter of
specimen had a significant effect (p<0.001) on the fracture load and
flexural strength. The highest flexural strength was obtained with the
control material (everStick, 1144.9+/-99.9 MPa). There was a linear
relationship between fracture load and diameter of posts for both glass
fiber and carbon fiber posts. Thermocycling decreased the flexural
modulus of the tested specimens by approximately 10%. Strength and
fracture load decreased approximately 18% as a result of thermocycling.SIGNIFICANCE: Considerable
variation can be found in the calculated strength values of the studied
post brands. Commercial prefabricated FRC posts showed lower flexural
properties than an individually polymerised FRC material.</div
Preparation of GHZ states via Grover's quantum searching algorithm
In this paper we propose an approach to prepare GHZ states of an arbitrary
multi-particle system in terms of Grover's fast quantum searching algorithm.
This approach can be regarded as an extension of the Grover's algorithm to
find one or more items in an unsorted database.Comment: 9 pages, Email address: [email protected]
The Ha luminosity function and star formation rate up to z~1
We describe ISAAC/ESO-VLT observations of the Ha(6563) Balmer line of 33
field galaxies from the Canada-France Redshift Survey (CFRS) with redshifts
selected between 0.5 and 1.1. We detect Ha in emission in 30 galaxies and
compare the properties of this sample with the low-redshift sample of CFRS
galaxies at z~0.2 (Tresse & Maddox 1998). We find that the Ha luminosity,
L(Ha), is tightly correlated to M(B(AB)) in the same way for both the low- and
high-redshift samples. L(Ha) is also correlated to L([OII]3727), and again the
relation appears to be similar at low and high redshifts. The ratio
L([OII])/L(Ha) decreases for brighter galaxies by as much as a factor 2 on
average. Derived from the Ha luminosity function, the comoving Ha luminosity
density increases by a factor 12 from =0.2 to =1.3. Our results confirm a
strong rise of the star formation rate (SFR) at z<1.3, proportional to
(1+z)^{4.1+/-0.3} (with H_0=50 km/s/Mpc, q_0=0.5). We find an average SFR(2800
Ang)/SFR(Ha) ratio of 3.2 using the Kennicutt (1998) SFR transformations. This
corresponds to the dust correction that is required to make the near UV data
consistent with the reddening-corrected Ha data within the self-contained,
I-selected CFRS sample.Comment: 16 pages, 16 figures and 3 tables included, figures and text updated,
same results as in the 1st version, accepted in MNRA
Decoherence of Einstein-Podolsky-Rosen pairs in a noisy Andreev entangler
We investigate quantum noise effect on the transportation of nonlocal Cooper
pairs accross the realistic Andreev entangler which consists of an s-wave
superconductor coupled to two small quantum dots at resonance which themselves
are coupled to normal leads. The noise emerges due to voltage fluctuations felt
by the electrons residing on the two dots as a result of the finite resistances
in the gate leads or of any resistive lead capacitively coupled to the dots. In
the ideal noiseless case, the setup provides a trustable source of mobile and
nonlocal spin-entangled electrons and the transport is dominated by a
two-particle Breit-Wigner resonance that allows the injection of two
spin-entangled electrons into different leads at the same energy [P. Recher, E.
V. Sukhorukov, and D. Loss, Phys. Rev. B 63, 165314 (2001)]. We seek to revisit
the transport of those nonlocal Cooper pairs as well as the efficiency of such
an Andreev entangler when including the quantum noise (decoherence).Comment: 15 pages and 6 figures; final version to appear in Physical Review
A New Spinel-Olivine Oxybarometer: Near-Liquidus Partitioning of V between Olivine-Melt, Spinel-Melt, and Spinel-Olivine in Martian Basalt Composition Y980459 as a Function of Oxygen Fugacity
Our research on valence state partitioning began in 2005 with a review of Cr, Fe, Ti, and V partitioning among crystallographic sites in olivine, pyroxene, and spinel [1]. That paper was followed by several on QUE94201 melt composition and specifically on Cr, V, and Eu partitioning between pyroxene and melt [2-5]. This paper represents the continuation of our examination of the partitioning of multivalent V between olivine, spinel, and melt in martian olivine-phyric basalts of Y980459 composition [6, 7]. Here we introduce a new, potentially powerful oxybarometer, V partitioning between spinel and olivine, which can be used when no melt is preserved in the meteorite. The bulk composition of QUE94201 was ideal for our study of martian pyroxene-phyric basalts and specifically the partitioning between pyroxene-melt for Cr, V, and Eu. Likewise, bulk composition Y980459 is ideal for the study of martian olivine-phyric basalts and specifically for olivine-melt, spinel-melt, and spinel-olivine partitioning of V as a function of oxygen fugacity
Star formation history of galaxies from z=0 to z=0.7 A backward approach to the evolution of star-forming galaxies
We investigate whether the mean star formation activity of star-forming
galaxies from z=0 to z=0.7 in the GOODS-S field can be reproduced by simple
evolution models of these systems. In this case, such models might be used as
first order references for studies at higher z to decipher when and to what
extent a secular evolution is sufficient to explain the star formation history
in galaxies.
We selected star-forming galaxies at z=0 and at z=0.7 in IR and in UV to have
access to all the recent star formation. We focused on galaxies with a stellar
mass ranging between 10^{10} and 10^{11} M_sun for which the results are not
biased by the selections. We compared the data to chemical evolution models
developed for spiral galaxies and originally built to reproduce the main
characteristics of the Milky Way and nearby spirals without fine-tuning them
for the present analysis. We find a shallow decrease in the specific star
formation rate (SSFR) when the stellar mass increases. The evolution of the
SSFR characterizing both UV and IR selected galaxies from z=0 to z=0.7 is
consistent with the models built to reproduce the present spiral galaxies.
There is no need to strongly modify of the physical conditions in galaxies to
explain the average evolution of their star formation from z=0 to z=0.7. We use
the models to predict the evolution of the star formation rate and the
metallicity on a wider range of redshift and we compare these predictions with
the results of semi-analytical models.Comment: 14 pages, 10 figures. accepted for publication in Astronomy &
Astrophysic
Valence State Partitioning of V between Pyroxene and Melt for Martian Melt Compositions Y 980459 and QUE 94201: The Effect of Pyroxene Composition and Crystal Structure
A spiked (with REE, V, Sc) martian basalt Y980459 composition was used to synthesize olivine, spinel, and pyroxene at 1200 C at 5 oxygen fugacities: IW-1, IW, IW+1, IW+2, and QFM. The high spike levels for REE were used for two specific reasons. First, we wanted to be able to analyze REE by both electron microprobe and ion probe. Second, we wanted the most important "Others" components, (i.e., those outside the pyroxene quadrilateral such as Al, Cr3+, Fe3+, REE3+, V3+, V4+, etc.) to be REE3+Mg (Si,Al)2O6. At the doped levels we used, the most important "Others" component is REE3+ in the M2 site coupled with Al in the tetrahedral site. The goal of this paper is to explain the significant increase in the value of D(sub V)(sup pyroxene/melt) with increased Wo content of the pyroxene. We compare augite (Wo approx. 33), pigeonite (Wo approx. 13) and orthopyroxene (Wo approx 3.8). We also show olivine for comparison. The crystal chemical factors which account for this remarkable increase of DV with Wo are twofold. First, with Ca in the M2 site (as in diopside, CaMgSi2O6) the site is large and 8-coordinated while Mg in the M2 site (as in enstatite, Mg2Si2O6) the site is smaller and 6- coordinated. Second, tetrahedral Al in the pyroxene chains provides charge balance and makes the M2 site larger and more compliant for the introduction of REE
Chromium Oxidation State in Planetary Basalts: Oxygen Fugacity Indicator and Critical Variable for Cr-Spinel Stability
Cr is a ubiquitous and relatively abundant minor element in basaltic, planetary magmas. At the reduced oxidation states (<FMQ) of many planetary basalts Cr is present in melts as both divalent and trivalent forms. The ratio of trivalent to divalent Cr present in the melt has many consequences for the stability and Cr concentration of magmatic phases such as spinel, clinopyroxene, and olivine. However, understanding the Cr valence in quenched melts has historically been plagued with analytical issues, and only recently has reliable methodology for quantifying Cr valence in quenched melts been developed. Despite this substantial difficulty, the pioneering works of Hanson and Jones and Berry and O'Neill provided important insights into the oxidation state of Cr in in silicate melts. Here we present a series of 1-bar gas mixing experiments performed with a Fe-rich basaltic melt in which have determined the Cr redox ratio of the melt at over a range of fO2 values by measuring this quantity in olivine with X-ray Absorption Near Edge Spectroscopy (XANES). The measured Cr redox ratio of the olivine phenocrysts can be readily converted to the ratio present in the conjugate melt via the ratio of crystal-liquid partition coefficients for Cr3+ and Cr2+. We have applied these results to modeling Cr spinel stability and Cr redox ratios in a primitive, iron-rich martian basalt
A List of Bright Interferometric Calibrators measured at the ESO VLTI
In a previous publication (Richichi & Percheron 2005) we described a program
of observations of candidate calibrator stars at the ESO Very Large Telescope
Interferometer (VLTI), and presented the main results from a statistical point
of view. In the present paper, we concentrate on establishing a new homogeneous
group of bright interferometric calibrators, based entirely on publicly
available K-band VLTI observations carried out with the VINCI instrument up to
July 2004. For this, we have defined a number of selection criteria for the
quality and volume of the observations, and we have accordingly selected a list
of 17 primary and 47 secondary calibrators. We have developed an approach to a
robust global fit for the angular diameters using the whole volume of
quality-controlled data, largely independent of a priori assumptions. Our
results have been compared with direct measurements, and indirect estimates
based on spectrophotometric methods, and general agreement is found within the
combined uncertainties. The stars in our list cover the range K=-2.9 to +3.0
mag in brightness, and 1.3 to 20.5 milliarcseconds in uniform-disk diameter.
The relative accuracy of the angular diameter values is on average 0.4% and 2%
for the primary and secondary calibrators respectively. Our calibrators are
well suited for interferometric observations in the near-infrared on baselines
between ~20m and ~200m, and their accuracy is superior, at least for the
primary calibrators, to other similar catalogues. Therefore, the present list
of calibrators has the potential to lead to significantly improved
interferometric scientific results
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